The Evolution of Radio Flux Density of Supernova Remnant G1.9+0.3 |
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| Affiliation: | 1. National Time Service Center, Chinese Academy of Sciences, Xi’an 710600;2. School of Electronic Electrical and Communication Engineering, University of Chinese Academy of Sciences, Beijing 100049;3. Key Laboratory of Precise Positioning and Timing Technology, Chinese Academy of Sciences, Xi’an 710600;4. Key Laboratory of Time and Frequency Primary Standards, Chinese Academy of Sciences, Xi’an 710600;1. School of Health Science and Engineering, University of Shanghai for Science and Technology, Shanghai 200093;2. Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030;3. Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Nanjing 210023;4. Shanghai Key Laboratory of Space Navigation and Position Techniques, Shanghai 20003;1. Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011 China;2. Xinjiang Key Laboratory of Microwave Technology, Urumqi 830011 China;3. School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, Beijing 100049 China;1. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023;2. School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026;3. Department of Astronomy, Xiamen University, Xiamen 361005;1. School of Physics and Astronomy, China West Normal University, Nanchong 637002;2. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023;3. Leibniz-Institute für Astrophysik Potsdam, Potsdam, D-14482 Germany;4. Department of Physics, Zhejiang University, Hangzhou 310058 |
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| Abstract: | Radio observations of young supernova remnants (SNRs) can shed light on the early evolution of SNRs. We selected G1.9+0.3 which is the youngest SNR in the Milky Way Galaxy for a study. We compiled the radio flux densities currently available and converted them to the same frequency, which leaves us the evolution of the flux density for the past nearly 50 years. We found that the flux density increased before 2008 and decreased afterwards, meaning the flux density reaching the maximum at an age of about 150–155 yr. We attributed the brightening of the SNR to the increase of either magnetic field or the accelerated high energy electrons. Based on the age at which the flux density reached the peak, combined with the previous numerical simulation, we discussed the ejecta mass of the supernova and kinetic energy released by the supernova explosion. |
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